A dataset provided by the European Space Agency

Name 067777
Title The ultimate XMM extragalactic survey [a]
URL

http://nxsa.esac.esa.int/nxsa-sl/servlet/data-action-aio?obsno=0677770101
http://nxsa.esac.esa.int/nxsa-sl/servlet/data-action-aio?obsno=0677770131
http://nxsa.esac.esa.int/nxsa-sl/servlet/data-action-aio?obsno=0677770132
http://nxsa.esac.esa.int/nxsa-sl/servlet/data-action-aio?obsno=0677770133
http://nxsa.esac.esa.int/nxsa-sl/servlet/data-action-aio?obsno=0677770134
http://nxsa.esac.esa.int/nxsa-sl/servlet/data-action-aio?obsno=0677770135
http://nxsa.esac.esa.int/nxsa-sl/servlet/data-action-aio?obsno=0677770136
http://nxsa.esac.esa.int/nxsa-sl/servlet/data-action-aio?obsno=0677770137
http://nxsa.esac.esa.int/nxsa-sl/servlet/data-action-aio?obsno=0677770138
http://nxsa.esac.esa.int/nxsa-sl/servlet/data-action-aio?obsno=0677770139
http://nxsa.esac.esa.int/nxsa-sl/servlet/data-action-aio?obsno=0677770140
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DOI 10.5270/esa-1s3bab8
Author Dr Marguerite Pierre
Description We propose a 10-40ks-field XMM survey over 50 deg2, designed to constrain the dark energy equation of state using the 600 - 1,400 clusters of galaxies that we will detect. The constraints that we will achieve on w_0 and w_a, of 0.7 and 2.4 (10ks coverage) and 0.4 and 1.2 (40ks coverage) are at the level of the ultimate Stage-IV DETF accuracy estimates achievable by cluster studies. This survey will also have lasting legacy value for cluster scaling laws and studies of AGN and XRB.
Publication The XXL Survey. I. Scientific motivations - XMM-Newton observing plan - Follow-up observations and simulation programme . Pierre, M., Pacaud, F., et all. . A&A . 592-1 . 2016 . 2016A&A...592A...1P ,
The XXL Survey. II. The bright cluster sample: catalogue and luminosity function . Pacaud, F., Clerc, N., et all. . A&A . 592-2 . 2016 . 2016A&A...592A...2P ,
The XXL Survey. III. Luminosity-temperature relation of the bright cluster sample . Giles, P. A., Maughan, B. J., et all. . A&A . 592-3 . 2016 . 2016A&A...592A...3G ,
The XXL Survey . IV. Mass-temperature relation of the bright cluster sample . Lieu, M., Smith, G. P., et all. . A&A . 592-4 . 2016 . 2016A&A...592A...4L ,
The XXL Survey. VI. The 1000 brightest X-ray point sources . Fotopoulou, S., Pacaud, F., et all. . A&A . 592-5 . 2016 . 2016A&A...592A...5F ,
The XXL Survey. VII. A supercluster of galaxies at z = 0.43 . Pompei, E., Adami, C., et all. . A&A . 592-6 . 2016 . 2016A&A...592A...6P ,
The XXL Survey. VIII. MUSE characterisation of intracluster light in a z ~ 0.53 cluster of galaxies . Adami, C., Pompei, E., et all. . A&A . 592-7 . 2016 . 2016A&A...592A...7A ,
The XXL Survey. XIII. Baryon content of the bright cluster sample . Eckert, D., Ettori, S., et all. . A&A . 592-12 . 2016 . 2016A&A...592A..12E ,
The XXL Survey. IX...
Instrument EMOS1, EMOS2, EPN, OM, RGS1, RGS2
Temporal Coverage 2012-05-21T03:44:05Z/2012-05-22T18:09:16Z
Version 17.56_20190403_1200
Mission Description The European Space Agency's (ESA) X-ray Multi-Mirror Mission (XMM-Newton) was launched by an Ariane 504 on December 10th 1999. XMM-Newton is ESA's second cornerstone of the Horizon 2000 Science Programme. It carries 3 high throughput X-ray telescopes with an unprecedented effective area, and an optical monitor, the first flown on a X-ray observatory. The large collecting area and ability to make long uninterrupted exposures provide highly sensitive observations.
Since Earth's atmosphere blocks out all X-rays, only a telescope in space can detect and study celestial X-ray sources. The XMM-Newton mission is helping scientists to solve a number of cosmic mysteries, ranging from the enigmatic black holes to the origins of the Universe itself. Observing time on XMM-Newton is being made available to the scientific community, applying for observational periods on a competitive basis.
Creator Contact https://www.cosmos.esa.int/web/xmm-newton/xmm-newton-helpdesk
Date Published 2012-06-01T00:00:00Z
Publisher And Registrant European Space Agency
Credit Guidelines European Space Agency, 2012-06-01T00:00:00Z, 067777, 17.56_20190403_1200. https://doi.org/10.5270/esa-1s3bab8